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Obliquity: a Probe for the Spin-Orbit Alignment and Formation History of Hot Jupiters

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Obliquity: a Probe for the Spin-Orbit Alignment and Formation History of Hot Jupiters Obliquity: A Probe for the Spin-Orbit Alignment and Formation History of Hot Jupiters A Thesis Presented by Caleb Cañas Submitted to The Department of Astronomy in partial fulfilment of the requirements for the degree of Bachelor of Arts Thesis Advisor: David Latham April 11, 2014 – 2 – Obliquity: A Probe for the Spin-Orbit Alignment and Formation History of Hot Jupiters Caleb Cañas ABSTRACT Hot Jupiters are intriguing because of their close proximity to the host star. Current theories have tried to explain their formation. However, these theories require knowledge of the obliquity, or the projected angle between the stellar spin vector and the orbital spin vector, for validation. In this thesis, I explore what the obliquity can inform us about the alignment between the planetary orbit and host star. I analyze the Rossiter-McLaughlin effect to derive the obliquity for two Hot Jupiter systems: HAT-P-49 and KELT-7. I use photometric data from KeplerCam to estimate stellar and systemic parameters. I use spectra from TRES and SOPHIE to estimate radial velocities and derive orbital solutions. For these systems, I adopt a simple model for the Rossiter-McLaughlin signature derived from geometry. I constrain the obliquity with this model using the MCMC analysis method. HAT-P-49b is a 1:7 MJ planet orbiting a 6820 K 1:5 M ˇ F-type star with a calculated obliquity of 90 17ı. KELT-7b is a hot ˙ Jupiter with a calculated obliquity of 8 17ı orbiting a 6780 K F-type star. ˙ I explore the possibility of constraining the obliquity for these systems using the rotational period, the stellar radius, and the projected rotational velocity of the host star. The potential for this second method is limited by the accuracy of the stellar parameters used. – 3 – Acknowledgements This thesis would not have been possible without the support and collaboration of many people. I would like to thank David Latham for his patience, guidance, and time during the past year. This was my first time researching in astrophysics and I am grateful forbeing introduced into the exciting world of exoplanets. Joshua Winn was another invaluable source for this project. His knowledge and guidance in all things Rossiter-McLaughlin helped make the analysis of HAT-P-49 and KELT-7b possible. I would like to thank Allyson Bieryla for her support, encouragement, and assistance with data management. I thank Lars Buchhave for providing the rotational velocities of KOI host stars and his knowledge on the derivation of the rotational velocities for stars. I thank the observers at Fred Lawrence Whipple Observatory who collected the data I used in this thesis. I would like to thank Jim Moran for giving me an opportunity to write a senior thesis despite being from a different concentration and for his insight, support and encouragement throughout year. I am grateful to my peers in Astronomy 99: Adrian Arteaga, Brian Claus, Diana Powell, and Natania Wolansky for their support and for making the year truly enjoyable. A shout out goes to my roommate, Chi Zeng, for his willingness to listen as work on my thesis progressed and for his optimism. Finally, I am grateful to friends and family, especially my mother, for their continuous support throughout my thesis and in everyday life. – 4 – Contents 1 The Importance of Extrasolar planets 7 1.1 A brief history on the quest for exoplanets . 8 1.2 Hot Jupiters: Enigmas in planetary formation . 9 1.2.1 Purported Migration of hot Jupiters . 10 1.3 Measuring Stellar obliquity . 17 1.3.1 The Rossiter-McLaughlin Effect . 17 1.3.2 Spectroscopy, Photometry, and Obliquity . 22 1.3.3 Asteroseismology and the Constraint on the Obliquity . 27 2 Observations 31 2.1 HAT-P-49b . 31 2.2 KELT-7b . 32 3 Obliquity from the Rossiter-McLaughlin Effect 33 3.1 HAT-P-49b: A Polar Hot Jupiter . 33 3.1.1 Validating the Residual Velocity of HAT-P-49b . 33 3.1.2 Modeling the RM Effect in HAT-P-49b . 34 3.1.3 Results and Discussion for HAT-P-49b . 40 3.2 KELT-7b: An Aligned Hot Jupiter . 41 3.2.1 Determining the Transit Parameters for KELT-7b . 41 – 5 – 3.2.2 Modeling the RM Effect in KELT-7b . 47 3.2.3 Results and Discussion for KELT-7b . 47 3.3 Improved Modeling of the RM Effect . 48 4 Constraining the Obliquity with Stellar & Transit Parameters 55 4.1 Required Parameters . 55 4.1.1 Stellar Parameters . 55 4.1.2 Spectroscopic Rotational Velocities . 56 4.1.3 Stellar Rotational Period . 57 4.2 Results . 58 4.2.1 Potential Error in the Stellar Radius . 58 4.2.2 Potential Error in the Rotational Period . 63 4.2.3 Potential Error in the Rotational Velocity . 65 5 Conclusion 66 5.1 Obliquity and the RM Effect . 66 5.2 Obliquity and Stellar Parameters . 68 5.3 The Obliquity and Exoplanetary Formation . 69 A The Radial Velocity Solution 71 A.1 Orbital Elements . 71 A.2 Deriving the Radial Velocity Solution . 73 – 6 – B Derivation of the Rossiter-McLaughlin Effect 74 B.1 The Geometry of a Transiting Extrasolar Planet . 74 B.2 Parameters for the system . 75 B.3 Analytical Approximation . 78 B.4 Addition Offset Velocity for HAT-P-49b & KELT-7b . 83 B.5 The semi-amplitude velocity as a free parameter for the RM Effect in HAT- P-49b & KELT-7b . 83 C Correlation Plots 85 C.1 HAT-P-49b . 85 C.2 KELT-7b . 85 D Markov Chain Monte Carlo Procedure for Uncertainties 85 References 89 – 7 – 1. The Importance of Extrasolar planets One of the questions humanity has always grappled with is about intelligent life elsewhere in the Universe. Is there another Earth somewhere in space? Throughout the centuries, particularly after the era of Greek philosophers, speculation about other worlds emerged and ranged from Aristotle’s assertion that “here cannot be more worlds than one” to Epicurius’ optimistic notion that “there are infinite worlds both like and unlike this world of ours”. Until recently it was impossible to confirm or refute any of these arguments. Fora long time, the only planetary system for study was the Solar System, from which subsequent theories about planetary formation and dynamics were derived. Fortunately, the recent discovery of extrasolar planets, or exoplanets, has been a boon to astronomers interested in planetary systems, their formation, their processes, habitability and, ultimately, about life elsewhere. Beginning in the early nineties, exoplanets were discovered using a variety of methods including the transit method, radial velocity method, astrometric measurement, direct imaging, and gravitational microlensing. As of this thesis, the NASA Exoplanet Archive lists 3845 Kepler candidates of interest and 1696 confirmed exoplanets. Of the 1696 confirmed exoplanets, most have been detected via the radial velocity method (503 exoplanets) or the transit method (1116 exoplanets). The radial velocity method was used to detect the first and exoplanet and looks for the host star’s reflex orbit due to the presence of a planet. The reflex orbit manifests itself as a perturbation in the radial velocity of the star.The transit method looks for a decrease in the light received from a system as a planet crosses in front of the disc of its host star. There are numerous transiting exoplanet surveys such as WASP, XO, CoRoT, TrES, and the well-known Kepler mission. All of these surveys aim to identify exoplanets and to improve models of planetary formation and dynamics. The goal of NASA’s Kepler mission was to observe transiting exoplanets in the search for Earth- – 8 – like candidates to give astronomers an idea of their frequency within the Milky Way. The Kepler mission has discovered a total of 964 confirmed exoplanets (from the NASA Exoplanet Archive). Astronomers have discovered exoplanetary systems with varying configurations and properties ranging from highly eccentric hot gaseous giants, exoplanets with turbulent evaporating atmospheres (Hébrard et al. 2004), and some with spectral lines suggesting a watery atmosphere (Swain et al. 2009; Deming et al. 2013). Recently, with the Kepler data, it has been speculated the Milky Way should host roughly forty billion planets with planets with the nearest Earth-like planet about four parsecs away (Petigura et al. 2013). 1.1. A brief history on the quest for exoplanets New instrumentation and techniques have revolutionized planetary discovery in the past decade. Before the nineties, the existence of exoplanets was purely theoretical. Long before the term exoplanet was in use, van de Kamp (1963) believed he discovered a companion to Barnard’s star. He used roughly fifty years of observations to build a case for an alleged companion with a mass of 1:6 MJ. At the time, this was such a novel concept that the New York Times declared there was another Solar System in our Universe. Years of scrutiny and observations failed to confirm the purported discovery and, recently, Choi et al. (2013) gave substantial evidence against the possibility of any planet around Barnard’s star and instead suggested it was purely geometric effect. Two of the earliest observations searching for exoplanets were performed separately by Bruce Campbell (Campbell et al. 1988) and by David Latham (Latham et al. 1989). While at the time these initial observations were not sufficient to prove the existence of exoplanets, they mark the start of a boom in exoplanetary discoveries. Campbell et al. observed slight perturbations in the radial velocity residuals, but dismissed it as activity in the Ca II emission line with a period comparable to those of the perturbations (Walker et al. 1992).
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